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19 results on '"Bouy, H."'

1. Euclid: Early Release Observations -- A glance at free-floating new-born planets in the sigma Orionis cluster

Author: Martín, E. L., {Ž}erjal, M., Bouy, H., Martin-Gonzalez, D., Torres, S. Mu{ň}oz, Barrado, D., Olivares, J., Pérez-Garrido, A., Mas-Buitrago, P., Cruz, P., Solano, E., Osorio, M. R. Zapatero, Lodieu, N., Béjar, V. J. S., Zhang, J. -Y., del Burgo, C., Huélamo, N., Laureijs, R., Mora, A., Saifollahi, T., Cuillandre, J. -C., Schirmer, M., Tata, R., Points, S., Phan-Bao, N., Goldman, B., Casewell, S. L., Reylé, C., Smart, R. L., Aghanim, N., Altieri, B., Andreon, S., Auricchio, N., Baldi, M., Balestra, A., Bardelli, S., Basset, A., Bender, R., Bonino, D., Branchini, E., Brescia, M., Brinchmann, J., Camera, S., Capobianco, V., Carbone, C., Carretero, J., Casas, S., Castellano, M., Cavuoti, S., Cimatti, A., Congedo, G., Conselice, C. J., Conversi, L., Copin, Y., Corcione, L., Courbin, F., Courtois, H. M., Cropper, M., Da Silva, A., Degaudenzi, H., Di Giorgio, A. M., Dinis, J., Dubath, F., Dupac, X., Dusini, S., Ealet, A., Farina, M., Farrens, S., Ferriol, S., Fosalba, P., Frailis, M., Franceschi, E., Fumana, M., Galeotta, S., Garilli, B., Gillard, W., Gillis, B., Giocoli, C., Gómez-Alvarez, P., Grazian, A., Grupp, F., Guzzo, L., Haugan, S. V. H., Hoar, J., Hoekstra, H., Holmes, W., Hook, I., Hormuth, F., Hornstrup, A., Hu, D., Hudelot, P., Jahnke, K., Jhabvala, M., Keihänen, E., Kermiche, S., Kiessling, A., Kilbinger, M., Kitching, T., Kohley, R., Kubik, B., Kümmel, M., Kunz, M., Kurki-Suonio, H., Mignant, D. Le, Ligori, S., Lilje, P. B., Lindholm, V., Lloro, I., Maino, D., Maiorano, E., Mansutti, O., Marggraf, O., Martinet, N., Marulli, F., Massey, R., Medinaceli, E., Mei, S., Melchior, M., Mellier, Y., Meneghetti, M., Meylan, G., Mohr, J. J., Moresco, M., Moscardini, L., Niemi, S. -M., Padilla, C., Paltani, S., Pasian, F., Pedersen, K., Percival, W. J., Pettorino, V., Pires, S., Polenta, G., Poncet, M., Popa, L. A., Pozzetti, L., Racca, G. D., Raison, F., Rebolo, R., Renzi, A., Rhodes, J., Riccio, G., Rix, Hans-Walter, Romelli, E., Roncarelli, M., Rossetti, E., Saglia, R., Sapone, D., Sartoris, B., Sauvage, M., Scaramella, R., Schneider, P., Secroun, A., Seidel, G., Seiffert, M., Serrano, S., Sirignano, C., Sirri, G., Stanco, L., Tallada-Crespí, P., Taylor, A. N., Teplitz, H. I., Tereno, I., Toledo-Moreo, R., Tsyganov, A., Tutusaus, I., Valenziano, L., Vassallo, T., Kleijn, G. Verdoes, Wang, Y., Weller, J., Williams, O. R., Zucca, E., Baccigalupi, C., Willis, G., Simon, P., Martín-Fleitas, J., and Scott, D.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: We provide an early assessment of the imaging capabilities of the Euclid space mission to probe deeply into nearby star-forming regions and associated very young open clusters, and in particular to check to what extent it can shed light on the new-born free-floating planet population. This paper focuses on a low-reddening region observed in just one Euclid pointing where the dust and gas has been cleared out by the hot sigma Orionis star. One late-M and six known spectroscopically confirmed L-type substellar members in the sigma Orionis cluster are used as benchmarks to provide a high-purity procedure to select new candidate members with Euclid. The exquisite angular resolution and depth delivered by the Euclid instruments allow us to focus on bona-fide point sources. A cleaned sample of sigma Orionis cluster substellar members has been produced and the initial mass function (IMF) has been estimated by combining Euclid and Gaia data. Our sigma Orionis substellar IMF is consistent with a power-law distribution with no significant steepening at the planetary-mass end. No evidence of a low-mass cutoff is found down to about 4 Jupiter masses at the young age (3 Myr) of the sigma Orionis open cluster., Comment: 13 pages, 10 figures, submitted to the A&A special issue on "Euclid on the sky"
Published: 2024

2. Searching for H$_{\alpha}$-emitting sources in the gaps of five transitional disks. SPHERE/ZIMPOL high-contrast imaging

Author: Huélamo, N., Chauvin, G., Mendigutía, I., Whelan, E., Alcalá, J. M., Cugno, G., Schmid, H. M., de Gregorio-Monsalvo, I., Zurlo, A., Barrado, D., Benisty, M., Quanz, S. P., Bouy, H., Montesinos, B., Beletsky, Y., and Szulagyi, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: (Pre-)transitional disks show gaps and cavities that can be related with on-going planet formation. According to theory, young embedded planets can accrete material from the circumplanetary and circumstellar disks, so that they could be detected in accretion tracers, like the H$_{\alpha}$ emission line. In this work, we present spectral angular differential imaging AO-assisted observations of five (pre-)transitional disks obtained with SPHERE/ZIMPOL at the Very Large Telescope (VLT). They were obtained in the H$_{\alpha}$ line and the adjacent continuum. We have combined spectral and angular differential imaging techniques to increase the contrast in the innermost regions close to the star, and search for the signature of young accreting protoplanets. As a result, the reduced images do not show any clear H$_{\alpha}$ point source around any of the targets. We report faint H$_{\alpha}$ emissions around TW Hya and HD163296: while the former is most probably an artifact related with a spike, the nature of the latter remains unclear. The spectral and angular differential images yield contrasts of 6--8 magnitudes at separations of $\sim$ 100 mas from the central stars, except in the case of LkCa15, with values of $\sim$3 mag. We have estimated upper limits to the accretion luminosity of potential protoplanets, obtaining that planetary models provide an average value of $L_{\rm acc} \sim 10^{-4}$ $L_{\odot}$ at 200 mas, which is $\sim$2 orders of magnitude higher than the $L_{\rm acc}$ estimated from the extrapolation of the $L_{H_{\alpha}}$ - $L_{acc}$ stellar relationship. We explain the lack of protoplanet detections as a combination of different factors, like e.g. episodic accretion, extinction from the circumstellar and circumplanetray disks, and/or a majority of low-mass, low-accreting planets., Comment: 17 pages, Accepted for publication in A&A
Published: 2022
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3. Infrared Spectroscopy of free-floating planet candidates in Upper Scorpius and Ophiuchus

Author: Bouy, H., Tamura, M., Barrado, D., Motohara, K., Rodríguez, N. Castro, Miret-Roig, N., Konishi, M., Koyama, S., Takahashi, H., Huelamo, N., Bertin, E., Olivares, J., Sarro, L. M., Berihuete, A., Cuillandre, J. -C., Galli, P. A. B., Yoshii, Y., and Miyata, T.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Context: A rich population of low-mass brown dwarfs and isolated planetary mass objects has been reported recently in the Upper Scorpius and Ophiuchus star forming complex. Aims: We investigate the membership, nature and properties of 17 of these isolated planetary mass candidates using low-resolution near-infrared spectra. Methods: We investigate the membership by looking for evidences of youth using four diagnostics: the slope of the continuum between the J and Ks band, the Hcont and TLI-g gravity sensitive indices, and by comparing the spectra to young and field (old) M and L-dwarf standards. Results: All the targets but one are confirmed as young ultracool objects, with spectral types between L0 and L6 and masses in the range 0.004-0.013 M according to evolutionary models. The status of the last target is unclear at this point. Conclusions: Only one possible contaminant has been identified among the 17 targets, suggesting that the contamination level of the original sample must be lower than 6%, Comment: Accepted on 2022 June 2. Pending language revision
Published: 2022
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4. Uncovering the ultimate planet impostor. An eclipsing brown dwarf in a hierarchical triple with two evolved stars

Author: Lillo-Box, J., Ribas, Á., Montesinos, B., Santos, N. C., Campante, T., Cunha, M., Barrado, D., Villaver, E., Sousa, S., Bouy, H., Aller, A., Corsaro, E., Li, T., Ong, J. M. J., Rebollido, I., Audenaert, J., and Pereira, F.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Exoplanet searches through space-based photometric time series have shown to be very efficient in recent years. However, follow-up efforts on the detected planet candidates have been demonstrated to be critical to uncover the true nature of the transiting objects. In this paper we show a detailed analysis of one of those false positives hidden as planetary signals. In this case, the candidate KOI-3886.01 showed clear evidence of a planetary nature from various techniques. Indeed, the properties of the fake planet set it among the most interesting and promising for the study of planetary evolution as the star leaves the main sequence. To unveil the true nature of this system, we present a complete set of observational techniques including high-spatial resolution imaging, high-precision photometric time series (showing eclipses, phase curve variations and asteroseismology signals), high-resolution spectroscopy and derived radial velocities, to unveil the true nature of this planet candidate. We find that KOI-3886.01 is an interesting false positive case: a hierarchical triple system composed by a $\sim$K2III giant star (KOI-3886A) accompanied by a close-in eclipsing binary formed by a subgiant $\sim$G4IV star (KOI-3886B) and a brown dwarf (KOI-3886C). In particular, KOI-3886C is one of the most irradiated brown dwarfs known to date, showing the largest radius in this substellar regime. It is also the first eclipsing brown dwarf known around an evolved star. In this paper we highlight the relevance of complete sets of follow-up observations to extrasolar planets detected by the transit technique using large-pixel photometers such as Kepler and TESS, and in the future, PLATO. In particular, multi-color high-spatial resolution imaging was the first hint toward ruling out the planet scenario in this system., Comment: Accepted for publication in A&A, 21 pages, 18 figures, 5 tables (language corrected version)
Published: 2021
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5. Dynamical traceback age of the $\beta$ Pictoris moving group

Author: Miret-Roig, N., Galli, P. A. B., Brandner, W., Bouy, H., Barrado, D., Olivares, J., Antoja, T., Romero-Gómez, M., Figueras, F., and Lillo-Box, J.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Context: The $\beta$ Pictoris moving group is one of the most well-known young associations in the solar neighbourhood and several members are known to host circumstellar discs, planets, and comets. Measuring its age with precision is basic to study several astrophysical processes such as planet formation and disc evolution which are strongly age dependent. Aims: We aim to determine a precise and accurate dynamical traceback age for the $\beta$ Pictoris moving group. Methods: Our sample combines the extremely precise Gaia DR2 astrometry with ground-based radial velocities measured in an homogeneous manner. We use an updated version of our algorithm to determine dynamical ages. The new approach takes into account a robust estimate of the spatial and kinematic covariance matrices of the association to improve the sample selection process and to perform the traceback analysis. Results: We estimate a dynamical age of $18.5_{-2.4}^{+2.0}$ Myr for the $\beta$ Pictoris moving group. We investigated the spatial substructure of the association at birth time and we propose the existence of a core of stars more concentrated. We also provide precise radial velocity measurements for 81 members of $\beta$ Pic, including ten stars with the first determination of their radial velocities. Conclusions: Our dynamical traceback age is three times more precise than previous traceback age estimates and, more important, for the first time, reconciles the traceback age with the most recent estimates of other dynamical, lithium depletion boundary, and isochronal ages. This has been possible thanks to the excellent astrometric and spectroscopic precisions, the homogeneity of our sample, and the detailed analysis of binaries and membership.
Published: 2020
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6. An optical transmission spectrum of the ultra-hot Jupiter WASP-33b. First indication of AlO in an exoplanet

Author: von Essen, C., Mallonn, M., Welbanks, L., Madhusudhan, N., Pinhas, A., Bouy, H., and Hansen, P. Weis
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: There has been increasing progress toward detailed characterization of exoplanetary atmospheres, in both observations and theoretical methods. Improvements in observational facilities and data reduction and analysis techniques are enabling increasingly higher quality spectra, especially from ground-based facilities. The high data quality also necessitates concomitant improvements in models required to interpret such data. In particular, the detection of trace species such as metal oxides has been challenging. Extremely irradiated exoplanets (~3000 K) are expected to show oxides with strong absorption signals in the optical. However, there are only a few hot Jupiters where such signatures have been reported. Here we aim to characterize the atmosphere of the ultra-hot Jupiter WASP-33b using two primary transits taken 18 orbits apart. Our atmospheric retrieval, performed on the combined data sets, provides initial constraints on the atmospheric composition of WASP-33b. We report a possible indication of aluminum oxide (AlO) at 3.3-sigma significance. The data were obtained with the long slit OSIRIS spectrograph mounted at the 10-meter Gran Telescopio Canarias. We cleaned the brightness variations from the light curves produced by stellar pulsations, and we determined the wavelength-dependent variability of the planetary radius caused by the atmospheric absorption of stellar light. A simultaneous fit to the two transit light curves allowed us to refine the transit parameters, and the common wavelength coverage between the two transits served to contrast our results. Future observations with HST as well as other large ground-based facilities will be able to further constrain the atmospheric chemical composition of the planet., Comment: 15 pages, 11 figures
Published: 2018
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7. Searching for H$_{\alpha}$ emitting sources around MWC758: SPHERE/ZIMPOL high-contrast imaging

Author: Huélamo, N., Chauvin, G., Schmid, H. M., Quanz, S. P., Whelan, E., Lillo-Box, J., Barrado, D., Montesinos, B., Alcalá, J. M., Benisty, M., de Gregorio-Monsalvo, I., Mendigutía, I., Bouy, H., Merín, B., de Boer, J., Garufi, A., and Pantin, E.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: MWC758 is a young star surrounded by a transitional disk. Recently, a protoplanet candidate has been detected around MWC758 through high-resolution $L'$-band observations. The candidate is located inside the disk cavity at a separation of $\sim$111 mas from the central star, and at an average position angle of $\sim$165.5 degrees. We have performed simultaneous adaptive optics observations of MWC758 in the H$_{\alpha}$ line and the adjacent continuum using SPHERE/ZIMPOL at the Very Large Telescope (VLT). We aim at detecting accreting protoplanet candidates through spectral angular differential imaging observations. The data analysis does not reveal any H$_{\alpha}$ signal around the target. The derived contrast curve in the B_Ha filter allows us to derive a 5$\sigma$ upper limit of $\sim$7.6 mag at 111 mas, the separation of the previously detected planet candidate. This contrast translates into a H$_{\alpha}$ line luminosity of $L_{\rm H_{\alpha}}\lesssim$ 5$\times$10$^{-5}$ $L_{\odot}$ at 111 mas, and an accretion luminosity of $L_{acc} <$3.7$\times$10$^{-4}\,L_{\odot}$. For the predicted mass range of MWC758b, 0.5-5 $M_{\rm Jup}$, this implies accretion rates of $\dot M \lesssim$ 3.4$\times$(10$^{-8}$-10$^{-9})\,M_{\odot}/yr$, for an average planet radius of 1.1 $R_{\rm Jup}$. Therefore, our estimates are consistent with the predictions of accreting circumplanetary accretion models for $R_{\rm in} = 1 R_{\rm Jup}$. In any case, the non-detection of any H$_{\alpha}$ emitting source in the ZIMPOL images does not allow us to unveil the true nature of the $L'$ detected source., Comment: 5 pages, accepted for publication in A&A letters
Published: 2018
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8. Mining the Kilo-Degree Survey for solar system objects

Author: Mahlke, M., Bouy, H., Altieri, B., Kleijn, G. Verdoes, Carry, B., Bertin, E., de Jong, J. T. A., Kuijken, K., McFarland, J., and Valentijn, E.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The search for minor bodies in the solar system promises insights into its formation history. Wide imaging surveys offer the opportunity to serendipitously discover and identify these traces of planetary formation and evolution. We aim to present a method to acquire position, photometry, and proper motion measurements of solar system objects in surveys using dithered image sequences. The application of this method on the Kilo-Degree Survey is demonstrated. Optical images of 346 square degree fields of the sky are searched in up to four filters using the AstrOmatic software suite to reduce the pixel to catalog data. The solar system objects within the acquired sources are selected based on a set of criteria depending on their number of observation, motion, and size. The Virtual Observatory SkyBoT tool is used to identify known objects. We observed 20,221 SSO candidates, with an estimated false-positive content of less than 0.05%. Of these SSO candidates, 53.4% are identified by SkyBoT. KiDS can detect previously unknown SSOs because of its depth and coverage at high ecliptic latitude, including parts of the Southern Hemisphere. Thus we expect the large fraction of the 46.6% of unidentified objects to be truly new SSOs. Our method is applicable to a variety of dithered surveys such as DES, LSST, and Euclid. It offers a quick and easy-to-implement search for solar system objects. SkyBoT can then be used to estimate the completeness of the recovered sample., Comment: Final version to be published in A&A. Supplementary data will be published at CDS. 11 pages, 15 figures
Published: 2017
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9. 280 one-opposition near-Earth asteroids recovered by the EURONEAR with the Isaac Newton Telescope

Author: Vaduvescu, O., Hudin, L., Mocnik, T., Char, F., Sonka, A., Tudor, V., Ordonez-Etxeberria, I., Alfaro, M. Diaz, Ashley, R., Errmann, R., Short, P., Moloceniuc, A., Cornea, R., Inceu, V., Zavoianu, D., Popescu, M., Curelaru, L., Mihalea, S., Stoian, A. -M., Boldea, A., Toma, R., Fields, L., Grigore, V., Stoev, H., Lopez-Martinez, F., Humphries, N., Sowicka, P., Ramanjooloo, Y., Manilla-Robles, A., Riddick, F. C., Jimenez-Lujan, F., Mendez, J., Aceituno, F., Sota, A., Jones, D., Hidalgo, S., Murabito, S., Oteo, I., Bongiovanni, A., Zamora, O., Pyrzas, S., Genova-Santos, R., Font, J., Bereciartua, A., Perez-Fournon, I., Martinez-Vazquez, C. E., Monelli, M., Cicuendez, L., Monteagudo, L., Agulli, I., Bouy, H., Huelamo, N., Monguio, M., Gansicke, B. T., Steeghs, D., Gentile-Fusillo, N. P., Hollands, M. A., Toloza, O., Manser, C. J., Dhillon, V., Sahman, D., Fitzsimmons, A., McNeill, A., Thompson, A., Tabor, M., Murphy, D. N. A., Davies, J., Snodgrass, C., Triaud, A. H. M. J., Groot, P. J., Macfarlane, S., Peletier, R., Sen, S., Ikiz, T., Hoekstra, H., Herbonnet, R., Kohlinger, F., Greimel, R., Afonso, A., Parker, Q. A., Kong, A. K. H., Bassa, C., and Pleunis, Z.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: One-opposition near-Earth asteroids (NEAs) are growing in number, and they must be recovered to prevent loss and mismatch risk, and to improve their orbits, as they are likely to be too faint for detection in shallow surveys at future apparitions. We aimed to recover more than half of the one-opposition NEAs recommended for observations by the Minor Planet Center (MPC) using the Isaac Newton Telescope (INT) in soft-override mode and some fractions of available D-nights. During about 130 hours in total between 2013 and 2016, we targeted 368 NEAs, among which 56 potentially hazardous asteroids (PHAs), observing 437 INT Wide Field Camera (WFC) fields and recovering 280 NEAs (76% of all targets). Engaging a core team of about ten students and amateurs, we used the THELI, Astrometrica, and the Find_Orb software to identify all moving objects using the blink and track-and-stack method for the faintest targets and plotting the positional uncertainty ellipse from NEODyS. Most targets and recovered objects had apparent magnitudes centered around V~22.8 mag, with some becoming as faint as V~24 mag. One hundred and three objects (representing 28% of all targets) were recovered by EURONEAR alone by Aug 2017. Orbital arcs were prolonged typically from a few weeks to a few years; our oldest recoveries reach 16 years. The O-C residuals for our 1,854 NEA astrometric positions show that most measurements cluster closely around the origin. In addition to the recovered NEAs, 22,000 positions of about 3,500 known minor planets and another 10,000 observations of about 1,500 unknown objects (mostly main-belt objects) were promptly reported to the MPC by our team. Four new NEAs were discovered serendipitously in the analyzed fields, increasing the counting to nine NEAs discovered by the EURONEAR in 2014 and 2015., Comment: Accepted for publication in Astronomy and Astrophysics (11 Oct 2017). Version 2 adding two co-authors and fixing the affiliation page overflow
Published: 2017
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10. Search for light curve modulations among Kepler candidates. Three very low-mass transiting companions

Author: Lillo-Box, J., Ribas, A., Barrado, D., Merín, B., and Bouy, H.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Light curve modulations in the sample of Kepler planet candidates allows the disentangling of the nature of the transiting object by photometrically measuring its mass. This is possible by detecting the effects of the gravitational pull of the companion (ellipsoidal modulations) and in some cases, the photometric imprints of the Doppler effect when observing in a broad band (Doppler beaming). We aim to photometrically unveil the nature of some transiting objects showing clear modulations in the phase-folded Kepler light curve. We selected a subsample among the large crop of Kepler objects of interest (KOIs) based on their chances to show detectable light curve modulations, i.e., close ($a<12~R_{\star}$) and large (in terms of radius) candidates. We modeled their phase-folded light curves with consistent equations for the three effects, namely, reflection, ellipsoidal and beaming (known as REB modulations). We provide detailed general equations for the fit of the REB modulations for the case of eccentric orbits. These equations are accurate to the photometric precisions achievable by current and forthcoming instruments and space missions. By using this mathematical apparatus, we find three close-in {very low-mass companions (two of them in the brown dwarf mass domain)} orbiting main-sequence stars (KOI-554, KOI-1074, and KOI-3728), and reject the planetary nature of the transiting objects (thus classifying them as false positives). In contrast, the detection of the REB modulations and transit/eclipse signal allows the measurement of their mass and radius that can provide important constraints for modeling their interiors since just a few cases of low-mass eclipsing binaries are known. Additionally, these new systems can help to constrain the similarities in the formation process of the more massive and close-in planets (hot Jupiters), brown dwarfs, and very low-mass companions., Comment: Accepted for publication in A&A on May 18th 2016, 9 pages, 5 figures, 4 tables. The first two authors contributed equally to the work contained in this paper
Published: 2016
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11. Constraining the properties of transitional disks in Chamaeleon I with Herschel

Author: Ribas, Á., Bouy, H., Merín, B., Duchêne, G., Rebollido, I., Espaillat, C., and Pinte, C.
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Transitional disks are protoplanetary disks with opacity gaps/cavities in their dust distribution, a feature that may be linked to planet formation. We perform Bayesian modeling of the three transitional disks SZ Cha, CS Cha and T25 including photometry from the Herschel Space Observatory to quantify the improvements added by these new data. We find disk dust masses between 2x10^-5 and 4x10^-4 Msun, and gap radii in the range of 7-18 AU, with uncertainties of ~ one order of magnitude and ~ 4 AU, respectively. Our results show that adding Herschel data can significantly improve these estimates with respect to mid-infrared data alone, which have roughly twice as large uncertainties on both disk mass and gap radius. We also find weak evidence for different density profiles with respect to full disks. These results open exciting new possibilities to study the distribution of disk masses for large samples of disks., Comment: 10 pages, 3 figures. Accepted for publication in MNRAS
Published: 2016
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12. Parallax of the L4.5 dwarf 2M1821$+$14 from high-precision astrometry with OSIRIS at GTC

Author: Sahlmann, J., Lazorenko, P. F., Bouy, H., Martín, E. L., Queloz, D., Ségransan, D., and Osorio, M. R. Zapatero
Subjects: Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We used the OSIRIS camera at the 10.4 m Gran Telescopio Canarias (GTC) to monitor the astrometric motion of the L4.5 dwarf 2M1821$+$14 over 17 months. The astrometric residuals of eleven epochs have a r.m.s. dispersion of 0.4 mas, which is larger than the average precision of 0.23 mas per epoch and hints towards an additional signal or excess noise. Comparison of the point-spread-functions in OSIRIS and FORS2/VLT images reveals no differences critical for high-precision astrometry, despite the GTC's segmented primary mirror. We attribute the excess noise to an unknown effect that may be uncovered with additional data. For 2M1821$+$14, we measured a relative parallax of $106.15 \pm 0.18$ mas and determined a correction of $0.50\pm0.05$ mas to absolute parallax, leading to a distance of $9.38 \pm0.03$ pc. We excluded at 3-$\sigma$ confidence the presence of a companion to 2M1821$+$14 down to a mass ratio of 0.1 ($\approx 5\, M_\mathrm{Jupiter}$) with a period of 50--1000 days and a separation of 0.1--0.7 au. The accurate parallax allowed us to estimate the age and mass of 2M1821$+$14 of 120--700 Myr and 0.049$^{+0.014}_{-0.024}$ M$_\odot$, thus confirming its intermediate age and substellar mass. We complement our study with a parallax and proper motion catalogue of 587 stars ($i'\simeq15.5-22$) close to 2M1821$+$14, used as astrometric references. This study demonstrates sub-mas astrometry with the GTC, a capability applicable for a variety of science cases including the search for extrasolar planets and relevant for future astrometric observations with E-ELT and TMT., Comment: 14 pages, 21 figures. Accepted for publication in MNRAS
Published: 2015
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13. The EChO science case

Author: Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Isaak, Kate, Linder, Martin, Lovis, Christophe, Micela, Giusi, Ollivier, Marc, Puig, Ludovic, Ribas, Ignasi, Snellen, Ignas, Allard, Bruce Swinyard. France, Barstow, Joanna, Cho, James, Coustenis, Athena, Cockell, Charles, Correia, Alexandre, Decin, Leen, de Kok, Remco, Deroo, Pieter, Encrenaz, Therese, Forget, Francois, Glasse, Alistair, Griffith, Caitlin, Guillot, Tristan, Koskinen, Tommi, Lammer, Helmut, Leconte, Jeremy, Maxted, Pierre, Mueller-Wodarg, Ingo, Nelson, Richard, North, Chris, Pallé, Enric, Pagano, Isabella, Piccioni, Guseppe, Pinfield, David, Selsis, Franck, Sozzetti, Alessandro, Stixrude, Lars, Tennyson, Jonathan, Turrini, Diego, Beaulieu, Mariarosa Zapatero-Osorio. Jean-Philippe, Grodent, Denis, Guedel, Manuel, Luz, David, Nørgaard-Nielsen, Hans Ulrik, Ray, Tom, Rickman, Hans, Selig, Avri, Banaszkiewicz, Mark Swain. Marek, Barlow, Mike, Bowles, Neil, Branduardi-Raymont, Graziella, Foresto, Vincent Coudé du, Gerard, Jean-Claude, Gizon, Laurent, Hornstrup, Allan, Jarchow, Christopher, Kerschbaum, Franz, Kovacs, Géza, Lagage, Pierre-Olivier, Lim, Tanya, Lopez-Morales, Mercedes, Malaguti, Giuseppe, Pace, Emanuele, Pascale, Enzo, Vandenbussche, Bart, Wright, Gillian, Adriani, Gonzalo Ramos Zapata. Alberto, Azzollini, Ruymán, Balado, Ana, Bryson, Ian, Burston, Raymond, Colomé, Josep, Crook, Martin, Di Giorgio, Anna, Griffin, Matt, Hoogeveen, Ruud, Ottensamer, Roland, Irshad, Ranah, Middleton, Kevin, Morgante, Gianluca, Pinsard, Frederic, Rataj, Mirek, Reess, Jean-Michel, Savini, Giorgio, Schrader, Jan-Rutger, Stamper, Richard, Abe, Berend Winter. L., Abreu, M., Achilleos, N., Ade, P., Adybekian, V., Affer, L., Agnor, C., Agundez, M., Alard, C., Alcala, J., Prieto, C. Allende, Floriano, F. J. Alonso, Altieri, F., Iglesias, C. A. Alvarez, Amado, P., Andersen, A., Aylward, A., Baffa, C., Bakos, G., Ballerini, P., Banaszkiewicz, M., Barber, R. J., Barrado, D., Barton, E. J., Batista, V., Bellucci, G., Avilés, J. A. Belmonte, Berry, D., Bézard, B., Biondi, D., Błęcka, M., Boisse, I., Bonfond, B., Bordé, P., Börner, P., Bouy, H., Brown, L., Buchhave, L., Budaj, J., Bulgarelli, A., Burleigh, M., Cabral, A., Capria, M. T., Cassan, A., Cavarroc, C., Cecchi-Pestellini, C., Cerulli, R., Chadney, J., Chamberlain, S., Charnoz, S., Jessen, N. Christian, Ciaravella, A., Claret, A., Claudi, R., Coates, A., Cole, R., Collura, A., Cordier, D., Covino, E., Danielski, C., Damasso, M., Deeg, H. J., Delgado-Mena, E., Del Vecchio, C., Demangeon, O., De Sio, A., De Wit, J., Dobrijévic, M., Doel, P., Dominic, C., Dorfi, E., Eales, S., Eiroa, C., Contreras, M. Espinoza, Esposito, M., Eymet, V., Fabrizio, N., Fernández, M., Castella, B. Femenía, Figueira, P., Filacchione, G., Fletcher, L., Focardi, M., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gambicorti, L., Gaulme, P., López, R. J. García, Garcia-Piquer, A., Gear, W., Gerard, J. -C., Gesa, L., Giani, E., Gianotti, F., Gillon, M., Giro, E., Giuranna, M., Gomez, H., Gomez-Leal, I., Hernandez, J. Gonzalez, Merino, B. González, Graczyk, R., Grassi, D., Guardia, J., Guio, P., Gustin, J., Hargrave, P., Haigh, J., Hébrard, E., Heiter, U., Heredero, R. L., Herrero, E., Hersant, F., Heyrovsky, D., Hollis, M., Hubert, B., Hueso, R., Israelian, G., Iro, N., Irwin, P., Jacquemoud, S., Jones, G., Jones, H., Justtanont, K., Kehoe, T., Kerschbaum, F., Kerins, E., Kervella, P., Kipping, D., Koskinen, T., Krupp, N., Lahav, O., Laken, B., Lanza, N., Lellouch, E., Leto, G., Goldaracena, J. Licandro, Lithgow-Bertelloni, C., Liu, S. J., Cicero, U. Lo, Lodieu, N., Lognonné, P., Lopez-Puertas, M., Lopez-Valverde, M. A., Rasmussen, I. Lundgaard, Luntzer, A., Machado, P., MacTavish, C., Maggio, A., Maillard, J. -P., Magnes, W., Maldonado, J., Mall, U., Marquette, J. -B., Mauskopf, P., Massi, F., Maurin, A. -S., Medvedev, A., Michaut, C., Miles-Paez, P., Montalto, M., Rodríguez, P. Montañés, Monteiro, M., Montes, D., Morais, H., Morales, J. C., Morales-Calderón, M., Morello, G., Martín, A. Moro, Moses, J., Bedon, A. Moya, Alcaino, F. Murgas, Oliva, E., Orton, G., Palla, F., Pancrazzi, M., Pantin, E., Parmentier, V., Parviainen, H., Ramírez, K. Y. Peña, Peralta, J., Perez-Hoyos, S., Petrov, R., Pezzuto, S., Pietrzak, R., Pilat-Lohinger, E., Piskunov, N., Prinja, R., Prisinzano, L., Polichtchouk, I., Poretti, E., Radioti, A., Ramos, A. A., Rank-Lüftinger, T., Read, P., Readorn, K., López, R. Rebolo, Rebordão, J., Rengel, M., Rezac, L., Rocchetto, M., Rodler, F., Béjar, V. J. Sánchez, Lavega, A. Sanchez, Sanromá, E., Santos, N., Forcada, J. Sanz, Scandariato, G., Schmider, F. -X., Scholz, A., Scuderi, S., Sethenadh, J., Shore, S., Showman, A., Sicardy, B., Sitek, P., Smith, A., Soret, L., Sousa, S., Stiepen, A., Stolarski, M., Strazzulla, G., Tabernero, H. M, Tanga, P., Tecsa, M., Temple, J., Terenzi, L., Tessenyi, M., Testi, L., Thompson, S., Thrastarson, H., Tingley, B. W., Trifoglio, M., Torres, J. Martín, Tozzi, A., Turrini, D., Varley, R., Vakili, F., de Val-Borro, M., Valdivieso, M. L., Venot, O., Villaver, E., Vinatier, S., Viti, S., Waldmann, I., Waltham, D., Ward-Thompson, D., Waters, R., Watkins, C., Watson, D., Wawer, P., Wawrzaszk, A., White, G., Widemann, T., Winek, W., Wiśniowski, T., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy
Published: 2015
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14. High-resolution imaging of $Kepler$ planet host candidates. A comprehensive comparison of different techniques

Author: Lillo-Box, J., Barrado, D., and Bouy, H.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Kepler mission has discovered thousands of planet candidates. Currently, some of them have already been discarded; more than 200 have been confirmed by follow-up observations, and several hundreds have been validated. However, most of them are still awaiting for confirmation. Thus, priorities (in terms of the probability of the candidate being a real planet) must be established for subsequent observations. The motivation of this work is to provide a set of isolated (good) host candidates to be further tested by other techniques. We identify close companions of the candidates that could have contaminated the light curve of the planet host. We used the AstraLux North instrument located at the 2.2 m telescope in the Calar Alto Observatory to obtain diffraction-limited images of 174 Kepler objects of interest. The lucky-imaging technique used in this work is compared to other AO and speckle imaging observations of Kepler planet host candidates. We define a new parameter, the blended source confidence level (BSC), to assess the probability of an object to have blended non-detected eclipsing binaries capable of producing the detected transit. We find that 67.2% of the observed Kepler hosts are isolated within our detectability limits, and 32.8% have at least one visual companion at angular separations below 6 arcsec. We find close companions (below 3 arcsec) for the 17.2% of the sample. The planet properties of this sample of non-isolated hosts are revised. We report one possible S-type binary (KOI-3158). We also report three possible false positives (KOIs 1230.01, 3649.01, and 3886.01) due to the presence of close companions. The BSC parameter is calculated for all the isolated targets and compared to both the value prior to any high-resolution image and, when possible, to observations from previous high-spatial resolution surveys in the Kepler sample., Comment: Accepted for publication in A&A on April 29, 2014; 32 pages, 11 figures, 11 tables
Published: 2014
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15. Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations

Author: Lillo-Box, J., Barrado, D., Moya, A., Montesinos, B., Montalbán, J., Bayo, A., Barbieri, M., Régulo, C., Mancini, L., Bouy, H., and Henning, T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The evolution of planetary systems is intimately linked to the evolution of their host star. Our understanding of the whole planetary evolution process is based on the large planet diversity observed so far. To date, only few tens of planets have been discovered orbiting stars ascending the Red Giant Branch. Although several theories have been proposed, the question of how planets die remains open due to the small number statistics. In this work we study the giant star Kepler-91 (KOI-2133) in order to determine the nature of a transiting companion. This system was detected by the Kepler Space Telescope. However, its planetary confirmation is needed. We confirm the planetary nature of the object transiting the star Kepler-91 by deriving a mass of $ M_p=0.88^{+0.17}_{-0.33} ~M_{\rm Jup}$ and a planetary radius of $R_p=1.384^{+0.011}_{-0.054} ~R_{\rm Jup}$. Asteroseismic analysis produces a stellar radius of $R_{\star}=6.30\pm 0.16 ~R_{\odot}$ and a mass of $M_{\star}=1.31\pm 0.10 ~ M_{\odot} $. We find that its eccentric orbit ($e=0.066^{+0.013}_{-0.017}$) is just $1.32^{+0.07}_{-0.22} ~ R_{\star}$ away from the stellar atmosphere at the pericenter. Kepler-91b could be the previous stage of the planet engulfment, recently detected for BD+48 740. Our estimations show that Kepler-91b will be swallowed by its host star in less than 55 Myr. Among the confirmed planets around giant stars, this is the planetary-mass body closest to its host star. At pericenter passage, the star subtends an angle of $48^{\circ}$, covering around 10% of the sky as seen from the planet. The planetary atmosphere seems to be inflated probably due to the high stellar irradiation., Comment: 21 pages, 8 tables and 11 figures
Published: 2013
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16. Characteristics and Large Bulk Density of the C-type Main-Belt Triple Asteroid (93) Minerva

Author: Marchis, F., Vachier, F., Ďurech, J., Enriquez, J. E., Harris, A. W., Dalba, P. A., Berthier, J., Emery, J. P., Bouy, H., Melbourne, J., Stockton, A., Fassnacht, C. D., Dupuy, T. J., and Strajnic, J.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: From a set of adaptive optics (AO) observations collected with the W.M. Keck telescope between August and September 2009, we derived the orbital parameters of the most recently discovered satellites of the large C-type asteroid (93) Minerva. The satellites of Minerva, which are approximately 3 and 4 km in diameter, orbit very close to the primary $\sim$5 & $\sim$8 $\times$ Rp and $\sim$1% & $\sim$2% $\times$ RHill) in a circular manner, sharing common characteristics with most of the triple asteroid systems in the main-belt. Combining these AO observations with lightcurve data collected since 1980 and two stellar occultations in 2010 & 2011, we removed the ambiguity of the pole solution of Minerva's primary and showed that it has an almost regular shape with an equivalent diameter Deq = 154 $\pm$ 6 km in agreement with IRAS observations. The surprisingly high bulk density of 1.75 $\pm$ 0.30 g/cm$\^3$ for this C-type asteroid, suggests that this taxonomic class is composed of asteroids with different compositions, For instance, Minerva could be made of the same material as dry CR, CO, and CV meteorites. We discuss possible scenarios on the origin of the system and conclude that future observations may shine light on the nature and composition of this fifth known triple main-belt asteroid., Comment: 35 pages, 9 figures, 5 tables
Published: 2013
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17. Identification of transitional disks in Chamaeleon with Herschel

Author: Ribas, Á., Merín, B., Bouy, H., de Oliveira, C. Alves, Ardila, D. R., Puga, E., Kóspál, Á., Spezzi, L., Cox, N. L. J., Prusti, T., Pilbratt, G. L., André, Ph., Matrà, L., and Vavrek, R.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract: Transitional disks are circumstellar disks with inner holes that in some cases are produced by planets and/or substellar companions in these systems. For this reason, these disks are extremely important for the study of planetary system formation. The Herschel Space Observatory provides an unique opportunity for studying the outer regions of protoplanetary disks. In this work we update previous knowledge on the transitional disks in the Chamaeleon I and II regions with data from the Herschel Gould Belt Survey. We propose a new method for transitional disk classification based on the WISE 12 micron-PACS 70 micron color, together with inspection of the Herschel images. We applied this method to the population of Class II sources in the Chamaeleon region and studied the spectral energy distributions of the transitional disks in the sample. We also built the median spectral energy distribution of Class II objects in these regions for comparison with transitional disks. The proposed method allows a clear separation of the known transitional disks from the Class II sources. We find 6 transitional disks, all previously known, and identify 5 objects previously thought to be transitional as possibly non-transitional. We find higher fluxes at the PACS wavelengths in the sample of transitional disks than those of Class II objects. We show the Herschel 70 micron band to be an efficient tool for transitional disk identification. The sensitivity and spatial resolution of Herschel reveals a significant contamination level among the previously identified transitional disk candidates for the two regions, which calls for a revision of previous samples of transitional disks in other regions. The systematic excess found at the PACS bands could be a result of the mechanism that produces the transitional phase, or an indication of different evolutionary paths for transitional disks and Class II sources., Comment: Accepted for publication in A&A: 11 March 2013 11 pages, 15 figures
Published: 2013
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18. Multiplicity in transiting planet host stars. A Lucky Imaging study of Kepler candidates

Author: Lillo-Box, J., Barrado, D., and Bouy, H.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: In the exoplanetary era, the Kepler spacecraft is causing a revolution by discovering thousands of new planet candidates. However, a follow up program is needed in order to reject false candidates and to fully characterize the bona-fide exoplanets. Our main aims are: 1./ Detect and analyze close companions inside the typical Kepler PSF to study if they are the responsible of the dim in the Kepler light curves, 2./ Study the change in the stellar and planetary parameters due to the presence of an unresolved object, 3./ Help to validate those Kepler Objects of Interest that do not present any object inside the Kepler PSF and 4./ Study the multiplicity rate in planet host candidates. Such a large sample of observed planet host candidates allows us to do statistics about the presence of close (visual or bounded) companions to the harboring star. We present here Lucky Imaging observations for a total amount of 98 Kepler Objects of Interest. This technique is based on the acquisition of thousands of very short exposure time images. Then, a selection and combination of a small amount of the best quality frames provides a high resolution image with objects having a 0.1 arcsec PSF. We applied this technique to carry out observations in the Sloan i and Sloan z filters of our Kepler candidates. We find blended objects inside the Kepler PSF for a significant percentage of KOIs. On one hand, only 58.2% of the hosts do not present any object within 6 arcsec. On the other hand, we have found 19 companions closer than 3 arcsec in 17 KOIs. According to their magnitudes and i-z color, 8 of them could be physically bounded to the host star., Comment: Accepted for publication in A&A on 01/08/2012, 18 pages, 8 figures and 8 tables. If you have problems with the quality of the figures, you can find a higher quality copy of this paper at http://www.cab.inta-csic.es/users/jlillo/Lillo-Box12_Kepler_LuckyImaging.pdf
Published: 2012
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19. The EChO science case

Author: Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Isaak, K., Linder, M., Lovis, C., Micela, G., Olliver, M., Puig, L., Ribas, I., De Sio, A., Frith, J., Justtanot, K., Showman, A., Alard, C., Yurchenko, S. N., Parviainen, H., Fouqué, P., Oliva, E., Bordé, P., Balado, A., Varley, R., Di Giorgio, A., Griffin, M., Maillard, J. P., Maggio, A., Lellouch, E., Strazzulla, G., Villaver, E., Griffith, C., Stamper, R., Amado, P. J., Rezac, L., Laken, B., Hargrave, P., Orton, G., Thompson, S., Morales, J. C., Wright, G., Massi, F., Lundgaard Rasmussen, I., Altieri, F., Covino, E., Coustenis, A., Moses, J., Lithgow Bertelloni, C., Demangeon, O., Fletcher, L., Morales Calderón, M., Lo Cicero, U., López Puertas, M., Capria, M. T., Danielski, C., Luntzer, A., Bulgarelli, A., González Hernández, J., Jacquemoud, S., MacTavish, C., Mall, U., Christian Jessen, N., Sanromá, E., Femenía Castella, B., Rocchetto, M., Miles Paez, P., Allard, F., Aylward, A., Leconte, J., Palla, F., White, G., Malaguti, G., Cavarroc, C., Lammer, H., Leto, G., Batista, V., Adybekian, V., Readorn, K., Polichtchouk, I., Petrov, R., García Piquer, A., Pancrazzi, M., Gómez Leal, I., Israelian, G., Rebolo López, R., Peralta, J., Giro, E., Tecsa, M., Haigh, J., Moro Martín, A., Pezzuto, S., Piskunov, N., Agnor, C., Hollis, M., Radioti, A., De Kok, R., Gear, W., Eymet, V., Achilleos, N., Koskinen, T., Maurin, A. S., Rank Lüftinger, T., Barlow, M., Figueira, P., Affer, L., Viti, S., Machado, P., Vakili, F., Burston, R., González Merino, B., Dominic, C., Dorfi, E., Smith, A., Sitek, P., Sánchez Lavega, A., Kerschbaum, F., Hoogeeven, R., Ballerini, P., Filacchione, G., Rodler, F., Stixrude, L., Parmentier, V., Del Val Borro, M., Vandenbussche, B., Tingley, B. W., Deeg, H. J., Tabernero, H. M., Shore, S., Fossey, S., Alonso Floriano, F. J., Santos, N., Tozzi, A., Kipping, D., Maruquette, J. B., Trifoglio, M., Scandaratio, G., Scuderi, S., Hébrard, E., Lodieu, N., Forget, F., Gustin, J., Poretti, E., Murgas Alcaino, F., Sicardy, B., Stiepen, A., Hubert, B., Grodent, D., Magnes, W., Tennyson, J., Temple, J., Galand, M., Barton, E. J., Winter, B., Valdivieso, M. L., Cordier, D., Heredero, R. L., Barrado, D., Mueller Wodarg, I., Giani, E., Correira, A., Widemann, T., Ward Thompson, D., Montañés Rodríguez, P., Moya Bedon, A., Venot, O., Prinja, R., Pinfield, D., Waldmann, I., Morello, G., Lim, T., Pallé, E., Waters, R., Wawer, P., Lognonné, P., Pietrzak, R., Fernández Hernández, Maite, Winek, W., Andersen, A., Monteiro, M., Liu, S. J., Rengel, M., Tanga, P., Yelle, R., Barstow, J. K., Maldonado, J., Irshad, R., Nelson, R., Colomé, J., De Witt, J., Lanza, N., Glasse, A., Coudé du Foresto, V., Branduardi Raymont, G., Beaulieu, J. P., Claudi, R., García López, Ramón, Eales, S., López Valverde, M. A., Turrini, D., Vinatier, S., Crook, J., Damasso, M., Ramos Zapata, G., Kovács, G., Banaszkiewicz, M., Focardi, M., Mauskopf, P., Guedel, M., Rebordao, J., Stolarski, M., Adriani, A., Norgaard Nielsen, H. U., Selig, A., Peña Ramírez, K. Y., Schmider, F. X., Baffa, C., Piccioni, G., Pantin, E., Bowles, N., Hornstrup, A., Pilat Lohinger, E., Buchhave, L. A., Soret, L., Börne, P., López Morales, M., Medvedev, A., Gesa, L., Jones, H., Pérez Hoyos, S., Gerard, J. C., Bellucci, G., Morais, H., Álvarez Iglesias, C. A., Abe, L., Pinsard, F., Tessenyi, M., Blecka, M., Wawrzaszk, A., Middleton, K., Martín Torres, J., Cho, J., Berry, D., Rataj, M., Schrader, J. R., Scholz, A., Watkins, C., Abreu, M., Testi, L., Decin, L., Sánz Forcada, J., Sozzetti, A., Lagage, P. O., Ade, P., Alcala, J., Sousa, S., Espinoza Contreras, M., Swinyard, B., Dobrijévic, M., Sánchez Béjar, V. J., Krupp, N., Bakos, G., Chamberlain, S., Chadney, J., Brown, L., Iro, N., Montalto, M., Sethenadh, J., Bouy, H., Ottensamer, R., Kehoe, T., Doel, P., Delgado Mena, E., Read, P., Coates, A., Cecchi Pestellini, C., Guillot, T., Budaj, J., Selsis, F., Jarchow, C., Del Vecchio, C., Cassan, A., Burleigh, M. R., Pagano, I., Ray, T., Gambicorti, L., Biondi, D., Cerulli, R., Ciaravella, A., Watson, D., Deroo, P., Collura, A., Graczyk, R., North, C., Ramos, A. A., Waltham, D., Montes, D., Gianotti, F., Thrastarson, H., Cockell, C., Pace, E., Bryson, I., Gómez, H., Esposito, M., Azzollini, R., Allende Prieto, C., Gillon, M., Fabrizio, N., Rickman, H., Rees, J. M., Pascale, E., Luzzi, D., Bonford, B., Cole, R., Gizon, L., Licandro Goldaracena, J., Agundez, M., Lahav, O., Zapatero Osorio, M. R., Gaulme, P., Encrenaz, T., Heyrovsky, D., Guàrdia, J., Prisinzano, L., Terenzi, L., Swain, M., Grassi, D., Eiroa, C., Maxted, P., Kerins, E., Yung, Y., Irwin, P., Herrero, E., Guio, P., Boisse, I., Claret, A., Kervella, P., Heiter, U., Bézard, B., Cabral, A., Michaut, C., Giuranna, M., Hersant, F., Hueso, R., Savini, G., Snellen, I. A., Charnoz, S., Jones, G., Belmonte Avilés, J. A., Barber, R. J., Wisniowski, T., Morgante, G., University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, U.S. Army Research Laboratory [Adelphi, MD] (ARL), United States Army (U.S. Army), Royal Observatory Edinburgh (ROE), University of Edinburgh, Departamento de Fisica [Aveiro], Universidade de Aveiro, SRON Netherlands Institute for Space Research (SRON), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Planetary Sciences [Tucson], University of Arizona, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), The Samuel Roberts Noble Foundation, Center for Human-Computer Interaction (HCI), Virginia Tech [Blacksburg], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), ECLIPSE 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCL London], Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), University of Stuttgart, Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Mullard Space Science Laboratory (MSSL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Curie [Paris], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Centre for Behaviour and Evolution, Institute of Neuroscience, Newcastle University [Newcastle], foreign laboratories (FL), CERN [Genève], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Estrutura de Missão para a Extensão da Plataforma Continental, Estrutura de Missão para a Extensão para a Extensão da Plataforma Continental, Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Queen Mary University of London (QMUL), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Department of Geoscience, Nelson Mandela University [Port Elizabeth], African Earth Observatory Network - Earth Stewardship Science Research Institute (AEON-ESSRI), Animal Genetics, Teagasc - The Agriculture and Food Development Authority (Teagasc), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Instituto Nacional de Engenharia, Tecnologia e Inovacao (INETI), Université Pierre et Marie Curie - Paris 6 (UPMC), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università di Salerno - Dipartimento di Matematica, Università degli Studi di Salerno = University of Salerno (UNISA), Department of Genetics, University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC)-Carolina Center for the Genome Sciences, Institut de Recerca i Tecnologia Agroalimentàries = Institute of Agrifood Research and Technology (IRTA), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Department of Molecular Medicine, Università degli Studi di Padova = University of Padua (Unipd), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), ASP 2015, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de génétique et microbiologie [Orsay] (IGM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH = German Research Center for Artificial Intelligence (DFKI), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Dipartimento di Matematica 'Ulisse Dini', Università degli Studi di Firenze = University of Florence (UniFI), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Université de Rennes (UR), Imperial College London, Laboratoire Hippolyte Fizeau (FIZEAU), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Bradford, Instituto Universitario de Electroquimica, Universidad de Alicante, Centre de recherche en éducation de Nantes (CREN), Le Mans Université (UM)-Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN), Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), NASA Goddard Space Flight Center (GSFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Los Alamos National Laboratory (LANL), Osserv Astrofis Catania, Ist Nazl Astrofis, Centre d'Etude de l'Energie Nucléaire (SCK-CEN), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Super Invest Cient, Inst Astrofis Andalucia, ES-18080 Granada, Spain, Department of Rheumatology (LEIDEN - Rhumato), Leiden University Medical Center (LUMC), Universiteit Leiden-Universiteit Leiden, Department of Rheumatology (COIMBRA - Rhumato), Universidade de Coimbra [Coimbra], Centre Scientifique et Technique du Bâtiment (CSTB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Université de Bordeaux (UB), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des gaz et des plasmas (LPGP), Pontificia Universidad Católica de Chile (UC), Department of Computer Science [Verona] (UNIVR | DI), Università degli studi di Verona = University of Verona (UNIVR), IEB-UNIVERSITY OF BARCELONA, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Thüringer Landessternwarte Tautenburg (TLS), Bremer Institut für Produktion und Logistik GmbH (BIBA), Universität Bremen, INAF - Osservatorio Astrofisico di Catania (OACT), Plasmon Nano-optics, Institut de Ciencies Fotoniques [Castelldefels] (ICFO), Royal Holloway [University of London] (RHUL), Hong Kong Government Environmental Protection Department, Water Policy and Science Group, National Space Agencies, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max Planck Institute for Solar System Research (MPS), European Space Agency (ESA), European Space Agency, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Samuel Roberts Noble Foundation, Inc., Universidade de Lisboa (ULISBOA), Polska Akademia Nauk (PAN), University of Oxford [Oxford], Max-Planck-Institut für Sonnensystemforschung (MPS), Institut Curie, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], AEON-ESSRI African Earth Observatory Network — Earth Stewardship Science Research Institute, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Physiologie de la reproduction et des comportements [Nouzilly] (PRC), Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Institut Français du Cheval et de l'Equitation [Saumur]-Institut National de la Recherche Agronomique (INRA), Université Francois Rabelais [Tours], Institut Français du Cheval et de l'Equitation, Università degli Studi di Salerno (UNISA), IRTA, Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH (DFKI), Universidade do Porto [Porto], Università degli Studi di Firenze [Firenze], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Department of Earth Sciences, University College London, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre interdisciplinaire de recherche, culture, éducation, formation, travail (CIRCEFT), Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Station biologique, Centre National de la Recherche Scientifique (CNRS), Dipartimento di Informatica [Verona], Università degli Studi di Verona, Departamento de Física e Astronomia [Porto], UMR5116, Centre Émile Durkheim (CED), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Clinica Neurologica, Università degli Studi di Perugia (UNIPG), Rebordao, J. [0000-0002-7418-0345], Kerschbaum, F. [0000-0001-6320-0980], Abreu, M. [0000-0002-0716-9568], Tabernero, H. [0000-0002-8087-4298], López Puertas, M. [0000-0003-2941-7734], Jacquemoud, S. [0000-0002-1500-5256], Tennyson, J. [0000-0002-4994-5238], Focardi, M. [0000-0002-3806-4283], Leto, G. [0000-0002-0040-5011], Lodieu, N. [0000-0002-3612-8968], Tinetti, G. [0000-0001-6058-6654], Sanroma, E. [0000-0001-8859-7937], Poretti, E. [0000-0003-1200-0473], Deeg, H. [0000-0003-0047-4241], Grassi, D. [0000-0003-1653-3066], Piccioni, G. [0000-0002-7893-6808], Ribas, I. [0000-0002-6689-0312], Coates, A. [0000-0002-6185-3125], García Ramón, J. [0000-0002-8204-6832], Bouy, H. [0000-0002-7084-487X[, Lognonne, P. [0000-0002-1014-920X], Demangeon, O. [0000-0001-7918-0355], Morales, J. C. [0000-0003-0061-518X], Ray, T. [0000-0002-2110-1068], Guio, P. [0000-0002-1607-5862], Tanga, P. [0000-0002-2718-997X], Prisinzano, L. [0000-0002-8893-2210], Barstow, J. [0000-0003-3726-5419], Balado, A. [0000-0003-4268-2516], Lithgow Bertelloni, C. [0000-0003-0924-6587], Barton, E. [0000-0001-5945-9244], Delgado, M. E. [0000-0003-4434-2195], Affer, L. [0000-0001-5600-3778], Ciaravella, A. [0000-0002-3127-8078], Barrado Navascues, D. [0000-0002-5971-9242], Figueira, P. [0000-0001-8504-283X], Covino, E. [0000-0002-6187-6685], Venot, O. [0000-0003-2854-765X], Cabral, A. [0000-0002-9433-871X], Watson, D. [0000-0002-4465-8264], Morales Calderon, M. [0000-0001-9526-9499], Ward Thompson, D. [0000-0003-1140-2761], Rebolo, R. [0000-0003-3767-7085], López Valverde, M. A. [0000-0002-7989-4267], Gillon, M. [0000-0003-1462-7739], Morgante, G. [0000-0001-9234-7412], Zapatero Osorio, M. R. [0000-0001-5664-2852], Bulgarelli, A. [0000-0001-6347-0649], Pena Ramírez, K. [0000-0002-5855-401X], Galand, M. [0000-0001-5797-914X], Pancrazzi, M. [0000-0002-3789-2482], Malaguti, G. [0000-0001-9872-3378], Sánchez Lavega, A. [0000-0001-7234-7634], Waldmann, I. [0000-0002-4205-5267], Kovacs, G. [0000-0002-2365-2330], Guillot, T. [0000-0002-7188-8428], Turrini, D. [0000-0002-1923-7740], Altieri, F. [0000-0002-6338-8300], Bellucci, G. [0000-0003-0867-8679], Baffa, C. [0000-0002-4935-100X], Olivia, E. [0000-0002-9123-0412], Selsis, F. [0000-0001-9619-5356], Scuderi, Salvatore [0000-0002-8637-2109], Hersant, F. [0000-0002-2687-7500], Gear, W. [0000-0001-6789-6196], Damasso, M. [0000-0001-9984-4278], Tizzi, A. [0000-0002-6725-3825], Pinfield, D. [0000-0002-7804-4260], Kipping, D. [0000-0002-4365-7366], Maldonado, J. [0000-0002-4282-1072], Pace, E. [0000-0001-5870-1772], Burleigh, M. [0000-0003-0684-7803], Monteiro, M. [0000-0001-5644-0898], Pilat Lohinger, E. [0000-0002-5292-1923], Chadney, J. [0000-0002-5174-2114], Moro Martín, A. [0000-0001-9504-8426], Claret, A. [0000-0002-4045-8134], Gómez, H. [0000-0003-3398-0052], Maldonado, J. [0000-0002-2218-5689], Michaut, C. [0000-0002-2578-0117], Hornstrup, A. [0000-0002-3363-0936], Scholz, A. [0000-0001-8993-5053], Irwin, P. [0000-0002-6772-384X], Bezard, B. [0000-0002-5433-5661], López Heredero, R. [0000-0002-2197-8388], Sanz Forcada, J. [0000-0002-1600-7835], Danielski, C. [0000-0002-3729-2663], Sousa, S. [0000-0001-9047-2965], Medved, A. [0000-0003-2713-8977], Bakos, G. [0000-0001-7204-6727], Ade, P. [0000-0002-5127-0401], Vandenbussche, B. [0000-0002-1368-3109], Martín Torres, J. [0000-0001-6479-2236], Correira, A. [0000-0002-8946-8579], Haigh, J. [0000-0001-5504-4754], Scandariato, G. [0000-0003-2029-0626], Guedel, M. [0000-0001-9818-0588], Sánchez Bejar, V. [0000-0002-5086-4232], Rodríguez, P. [0000-0002-6855-9682], Piskunov, N. [0000-0001-5742-7767], Adibekyan, V. [0000-0002-0601-6199], Pérez Hoyos, S. [0000-0001-9797-4917], Kervella, P. [0000-0003-0626-1749], Pascale, E. [0000-0002-3242-8154], Claudi, R. [0000-0001-7707-5105], Filacchione, G. [0000-0001-9567-0055], Rickman, H. [0000-0002-9603-6619], Amado, P. J. [0000-0002-8388-6040], Maggio, A. [0000-0001-5154-6108], Agundez, M. [0000-0003-3248-3564], Montes, D. [0000-0002-7779-238X], Fletcher, L. [0000-0001-5834-9588], Stixrude, L. [0000-0003-3778-2432], Morais, M. H. [0000-0001-5333-2736], Hueso, R. [0000-0003-0169-123X], Yurchenko, S. [0000-0001-9286-9501], Rataj, M. [0000-0002-2978-9629], Pérez Hoyos, S. [0000-0002-2587-4682], Santos, N. [0000-0003-4422-2919], Peralta, J. [0000-0002-6823-1695], Budaj, J. [0000-0002-9125-7340], Barlow, M. [0000-0002-3875-1171], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto, Università degli Studi di Firenze = University of Florence [Firenze] (UNIFI), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), University of Verona (UNIVR), Universidade do Porto-Universidade do Porto, Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN)-Le Mans Université (UM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), Institut National de la Recherche Agronomique (INRA)-Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Firenze = University of Florence [Firenze], COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, University College of London [London] ( UCL ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Max Planck Institute for Solar System Research ( MPS ), School of Physics & Astronomy, European Space Agency ( ESA ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire des technologies de la microélectronique ( LTM ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Microélectronique, Electromagnétisme et Photonique - Laboratoire d'Hyperfréquences et Caractérisation ( IMEP-LAHC ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut National Polytechnique de Grenoble ( INPG ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Universidad Politécnica de Cataluña, U.S. Army Research Laboratory [Adelphi, MD] ( ARL ), United States Army ( U.S. Army ), Royal Observatory Edinburgh ( ROE ), SRON Netherlands Institute for Space Research ( SRON ), Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Lunar and Planetary Laboratory [Tucson], Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Center for Human-Computer Interaction ( HCI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), University of Hertfordshire [Hatfield] ( UH ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Atmosphérique et Planétaire ( LPAP ), Centro de Astronomia e Astrofísica da Universidade de Lisboa ( CAAUL ), Universidade de Lisboa ( ULISBOA ), Space Research Centre [Warsaw] ( CBK ), Polska Akademia Nauk ( PAN ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), Mullard Space Science Laboratory ( MSSL ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven ( KU Leuven ), foreign laboratories ( FL ), STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Centre for Planetary Sciences [UCL/Birkbeck] ( CPS ), Queen Mary University of London ( QMUL ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Dark Cosmology Center, Niels Bohr Institute, University of Copenhagen ( KU ), Computational Science and Engineering Department [Daresbury] ( STFC ), LAEX, Depto. Astrofísica, Centro de Astrobiología, Nelson Mandela Metropolitan University, Nelson Mandela Metropolitan University [Port Elizabeth, South Africa]-Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], Teagasc, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Fraunhofer-Institute for Applied Solid-State Physics (IAF), Centro de Astrobiologia [Madrid] ( CAB ), Instituto Nacional de Técnica Aeroespacial ( INTA ) -Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Instituto Nacional de Engenharia, Tecnologia e Inovacco ( INETI ), INETI, Université Pierre et Marie Curie - Paris 6 ( UPMC ), Physiologie de la reproduction et des comportements [Nouzilly] ( PRC ), Institut National de la Recherche Agronomique ( INRA ) -Institut Français du Cheval et de l'Equitation [Saumur]-Université de Tours-Centre National de la Recherche Scientifique ( CNRS ), Università degli Studi di Salerno ( UNISA ), The University of North Carolina at Chapel Hill-Carolina Center for the Genome Sciences, Laboratoire d'astrophysique de l'observatoire de Besançon ( LAOB ), Université de Franche-Comté ( UFC ), Universita degli Studi di Padova = University of Padua = Université de Padoue, Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Institut de génétique et microbiologie [Orsay] ( IGM ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH ( DFKI ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ), Laboratoire Hippolyte Fizeau ( FIZEAU ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Istituto di Fisica dello Spazio Interplanetario CNR (IFSI), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de recherche en éducation de Nantes ( CREN ), Université de Nantes ( UN ), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea ( UPV/EHU ), NASA Goddard Space Flight Center ( GSFC ), Onsala Space Observatory ( OSO ), Los Alamos National Laboratory ( LANL ), Centre d'Etude de l'Energie Nucléaire ( SCK-CEN ), Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Rheumatology ( LEIDEN - Rhumato ), Department of Rheumatology ( COIMBRA - Rhumato ), Centre Scientifique et Technique du Bâtiment ( CSTB ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Centre interdisciplinaire de recherche, culture, éducation, formation, travail ( CIRCEFT ), Université Paris 8 Vincennes-Saint-Denis ( UP8 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique des gaz et des plasmas ( LPGP ), Pontificia Universidad Católica de Chile, Thüringer Landessternwarte Tautenburg ( TLS ), BIBA Bremer Institut für Produktion und Logistik GmbH, Centre Émile Durkheim ( CED ), Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Institut de Ciencies Fotoniques [Castelldefels] ( ICFO ), Università di Perugia, Royal Holloway [University of London] ( RHUL ), and Low Energy Astrophysics (API, FNWI)
Subjects: Astrofísica, Solar System, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], HOT-JUPITER ATMOSPHERES, 7. Clean energy, Space missions, law.invention, Astronomi, astrofysik och kosmologi, Planet, law, Observatory, Astronomy, Astrophysics and Cosmology, Transit (astronomy), Atmospheric science, Exoplanets, IR astronomy, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, QC, QB, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, GIANT PLANETS, Physical Sciences, ENERGY-BALANCE, Astrophysics::Earth and Planetary Astrophysics, Population, MU-M, FOS: Physical sciences, F500, Astronomy & Astrophysics, Telescope, INFRARED-EMISSION-SPECTRUM, education, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], EXTRASOLAR PLANET ATMOSPHERE, Science & Technology, Astronomy, EXOPLANET HD 189733B, HUBBLE-SPACE-TELESCOPE, Astronomía, TRANSMISSION SPECTROSCOPY, 0201 Astronomical And Space Sciences, 13. Climate action, WATER-VAPOR, astro-ph.EP, Astrophysics - Earth and Planetary Astrophysics
Abstract: The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy
Published: 2015

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19 results on '"Bouy, H."'

1. Euclid: Early Release Observations -- A glance at free-floating new-born planets in the sigma Orionis cluster

2. Searching for H$_{\alpha}$-emitting sources in the gaps of five transitional disks. SPHERE/ZIMPOL high-contrast imaging

3. Infrared Spectroscopy of free-floating planet candidates in Upper Scorpius and Ophiuchus

4. Uncovering the ultimate planet impostor. An eclipsing brown dwarf in a hierarchical triple with two evolved stars

5. Dynamical traceback age of the $\beta$ Pictoris moving group

6. An optical transmission spectrum of the ultra-hot Jupiter WASP-33b. First indication of AlO in an exoplanet

7. Searching for H$_{\alpha}$ emitting sources around MWC758: SPHERE/ZIMPOL high-contrast imaging

8. Mining the Kilo-Degree Survey for solar system objects

9. 280 one-opposition near-Earth asteroids recovered by the EURONEAR with the Isaac Newton Telescope

10. Search for light curve modulations among Kepler candidates. Three very low-mass transiting companions

11. Constraining the properties of transitional disks in Chamaeleon I with Herschel

12. Parallax of the L4.5 dwarf 2M1821$+$14 from high-precision astrometry with OSIRIS at GTC

13. The EChO science case

14. High-resolution imaging of $Kepler$ planet host candidates. A comprehensive comparison of different techniques

15. Kepler-91b: a planet at the end of its life. Planet and giant host star properties via light-curve variations

16. Characteristics and Large Bulk Density of the C-type Main-Belt Triple Asteroid (93) Minerva

17. Identification of transitional disks in Chamaeleon with Herschel

18. Multiplicity in transiting planet host stars. A Lucky Imaging study of Kepler candidates

19. The EChO science case

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